Similarities and Differences between ICME-driven Shocks Observed by VEX (∼0.72 au) and WIND (∼1.0 au)
The features of interplanetary shocks driven by interplanetary coronal mass ejections (ICMEs) observed by WIND (∼1.0 au) and Venus Express (VEX; ∼0.72 au) during the same period are statistically analyzed by comparing their similarities and differences. It is found that the proportion of ICME-driven...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ada35b |
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| author | Mengsi Ruan Pingbing Zuo Zilu Zhou Jiayun Wei Xueshang Feng Yi Wang Qi Xu Xiaojun Xu Zhengyang Zou Zhenning Shen |
| author_facet | Mengsi Ruan Pingbing Zuo Zilu Zhou Jiayun Wei Xueshang Feng Yi Wang Qi Xu Xiaojun Xu Zhengyang Zou Zhenning Shen |
| author_sort | Mengsi Ruan |
| collection | DOAJ |
| description | The features of interplanetary shocks driven by interplanetary coronal mass ejections (ICMEs) observed by WIND (∼1.0 au) and Venus Express (VEX; ∼0.72 au) during the same period are statistically analyzed by comparing their similarities and differences. It is found that the proportion of ICME-driven shocks in all shocks decreases slightly from ∼0.72 to ∼1 au. The yearly occurrence of ICME-driven shocks at both ∼0.72 and ∼1 au roughly follows the sunspot cycle, while the magnetic field ratio does not show such a correspondence. In each year, the annual medians of the shock angle for ICME-driven shocks at ∼1 au are consistently larger than those at ∼0.72 au, and the annual medians of the magnetic field ratio for events at ∼1 au are slightly smaller than those at ∼0.72 au. Planar magnetic structures (PMSs) downstream of ICME-driven shocks are also analyzed. Approximately 28.57% of the detected PMS events from VEX observations and 28.84% from WIND observations cover the entire 2 hr intervals downstream of the shocks, which are referred to as full PMS events. Through comparative analysis for VEX and WIND observations, it is found that strong and quasi-perpendicular ICME-driven shocks are the most preferable conditions for full PMS formation. |
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| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-a6343d8043d64d97945b4a79703ba3122025-01-30T12:29:49ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-019801910.3847/1538-4357/ada35bSimilarities and Differences between ICME-driven Shocks Observed by VEX (∼0.72 au) and WIND (∼1.0 au)Mengsi Ruan0Pingbing Zuo1https://orcid.org/0000-0003-4711-0306Zilu Zhou2https://orcid.org/0000-0002-4463-8407Jiayun Wei3https://orcid.org/0000-0001-8720-5962Xueshang Feng4https://orcid.org/0000-0001-8605-2159Yi Wang5https://orcid.org/0000-0002-7094-9794Qi Xu6Xiaojun Xu7https://orcid.org/0000-0002-2309-0649Zhengyang Zou8https://orcid.org/0000-0003-1273-4573Zhenning Shen9https://orcid.org/0000-0002-4148-8044Shenzhen Key Laboratory of Numerical Prediction for Space Storm, School of Aerospace, Harbin Institute of Technology , Shenzhen 518055, People’s Republic of China ; pbzuo@hit.edu.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of ChinaShenzhen Key Laboratory of Numerical Prediction for Space Storm, School of Aerospace, Harbin Institute of Technology , Shenzhen 518055, People’s Republic of China ; pbzuo@hit.edu.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of ChinaState Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology , Macao 999078, People’s Republic of ChinaShenzhen Key Laboratory of Numerical Prediction for Space Storm, School of Aerospace, Harbin Institute of Technology , Shenzhen 518055, People’s Republic of China ; pbzuo@hit.edu.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of ChinaShenzhen Key Laboratory of Numerical Prediction for Space Storm, School of Aerospace, Harbin Institute of Technology , Shenzhen 518055, People’s Republic of China ; pbzuo@hit.edu.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of ChinaShenzhen Key Laboratory of Numerical Prediction for Space Storm, School of Aerospace, Harbin Institute of Technology , Shenzhen 518055, People’s Republic of China ; pbzuo@hit.edu.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of ChinaKey Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of ChinaState Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology , Macao 999078, People’s Republic of ChinaState Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology , Macao 999078, People’s Republic of ChinaState Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology , Macao 999078, People’s Republic of ChinaThe features of interplanetary shocks driven by interplanetary coronal mass ejections (ICMEs) observed by WIND (∼1.0 au) and Venus Express (VEX; ∼0.72 au) during the same period are statistically analyzed by comparing their similarities and differences. It is found that the proportion of ICME-driven shocks in all shocks decreases slightly from ∼0.72 to ∼1 au. The yearly occurrence of ICME-driven shocks at both ∼0.72 and ∼1 au roughly follows the sunspot cycle, while the magnetic field ratio does not show such a correspondence. In each year, the annual medians of the shock angle for ICME-driven shocks at ∼1 au are consistently larger than those at ∼0.72 au, and the annual medians of the magnetic field ratio for events at ∼1 au are slightly smaller than those at ∼0.72 au. Planar magnetic structures (PMSs) downstream of ICME-driven shocks are also analyzed. Approximately 28.57% of the detected PMS events from VEX observations and 28.84% from WIND observations cover the entire 2 hr intervals downstream of the shocks, which are referred to as full PMS events. Through comparative analysis for VEX and WIND observations, it is found that strong and quasi-perpendicular ICME-driven shocks are the most preferable conditions for full PMS formation.https://doi.org/10.3847/1538-4357/ada35bInterplanetary shocksAstronomy data analysisSolar coronal mass ejectionsInterplanetary magnetic fields |
| spellingShingle | Mengsi Ruan Pingbing Zuo Zilu Zhou Jiayun Wei Xueshang Feng Yi Wang Qi Xu Xiaojun Xu Zhengyang Zou Zhenning Shen Similarities and Differences between ICME-driven Shocks Observed by VEX (∼0.72 au) and WIND (∼1.0 au) The Astrophysical Journal Interplanetary shocks Astronomy data analysis Solar coronal mass ejections Interplanetary magnetic fields |
| title | Similarities and Differences between ICME-driven Shocks Observed by VEX (∼0.72 au) and WIND (∼1.0 au) |
| title_full | Similarities and Differences between ICME-driven Shocks Observed by VEX (∼0.72 au) and WIND (∼1.0 au) |
| title_fullStr | Similarities and Differences between ICME-driven Shocks Observed by VEX (∼0.72 au) and WIND (∼1.0 au) |
| title_full_unstemmed | Similarities and Differences between ICME-driven Shocks Observed by VEX (∼0.72 au) and WIND (∼1.0 au) |
| title_short | Similarities and Differences between ICME-driven Shocks Observed by VEX (∼0.72 au) and WIND (∼1.0 au) |
| title_sort | similarities and differences between icme driven shocks observed by vex ∼0 72 au and wind ∼1 0 au |
| topic | Interplanetary shocks Astronomy data analysis Solar coronal mass ejections Interplanetary magnetic fields |
| url | https://doi.org/10.3847/1538-4357/ada35b |
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